Uh neutrino initiatives projects
Download
1 / 15

UH Neutrino Initiatives & Projects - PowerPoint PPT Presentation


  • 78 Views
  • Uploaded on

UH Neutrino Initiatives & Projects. Low (MeV) Energy, ongoing (1000-25000 tons): Super-Kamiokande: solar & atmospheric KamLAND: reactor & solar High & Ultra-high Energy (PeV to ZeV): 10-1000km^3 ANITA: NASA long duration balloon GLUE: ongoing, using NASA Deep space network

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

PowerPoint Slideshow about ' UH Neutrino Initiatives & Projects' - ziva


An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
Uh neutrino initiatives projects
UH Neutrino Initiatives & Projects

  • Low (MeV) Energy, ongoing (1000-25000 tons):

    • Super-Kamiokande: solar & atmospheric

    • KamLAND: reactor & solar

  • High & Ultra-high Energy (PeV to ZeV): 10-1000km^3

    • ANITA: NASA long duration balloon

    • GLUE: ongoing, using NASA Deep space network

    • FORTE: DOE satellite, sensitive to UHE neutrinos

    • ASHRA: air shower + tau neutrinos

    • SalSA: a next generation underground detector


Super kamiokande biggest current underground detector rebuilt in 2002 to density of pmts
Super-Kamiokande Biggest Current Underground νDetectorrebuilt in 2002 to ½ density of PMTs

  • Since Apr. ’96, >1400 days

  • 22,500 ton fiducial Vol.

  • 1,200 m2 muon area

  • 4 MeV – 200 GeV evts

  • SuperK shows Strong evidence for

    νµ↔ντ oscillations

    ▫ Neutrino Mass!!!

ICRR, U-Tokyo


But neutrino astronomy began with solar neutrinos 30 yrs ago
But Neutrino Astronomy Began withSolar Neutrinos 30 Yrs Ago!

• SK Portrait of the Sun

in Neutrinos

• Data from Homestake,

SAGE, GALLEX/GNO,

Kamioka, SuperK, SNO

• But Flux Only ~1/2-1/3

of Expectations

R. Svoboda, LSU


Kamland taking data first results 12 02
KamLANDtaking data, first results 12/02

•Measure νe’s from reactors in Japan at

~175 km distance.

•Makes terrestrial measurement.

KamLAND


Kamland first results
KamLAND First Results

Final sample 54 events

(Eprompt > 2.6MeV )

Predicted 86.8 ± 5.6 events

(no osc)

Background 0.95 ± 0.99 events

accidental 0.0086 ± 0.0005

9Li/8He 0.94 ± 0.85

fast neutron < 0.5

(Nobs- Nbgd)/Npred = 0.611 ± 0.085 (stat)

± 0.041 (syst)


Detecting the TeV to EeV Cascades:

Radio vs. Optical

  • Radio Cherenkov:

    • broad spectrum,

  • few MHz to ~10 GHz.

    • intensity: Power ~ (Energy)2,

    • thermal noise constant.

    • SNR >1 at >PeV energies

    • for ~100 m range.

    • •needs radio-clear medium -

    • cold ice or dry rock

  • For >>PeV cascade detection,

    • radio favored over optical.

P. Gorham


Goldstone lunar ultra high energy neutrino experiment glue similar activity starting in russia
Goldstone Lunar Ultra-high energy neutrino Experiment (GLUE)[Similar activity starting in Russia]


NASA Goldstone Radio Detection Approach

RF pulse spectrum & shape

  • Effective target volume: antenna beam (~0.3 deg) times ~10 m layer

    => ~100,000 cubic km !

  • Limited primarily by livetime - small portion of antenna time devoted to any single project.


Forte an existing space based ehe neutrino cosmic ray radio detector
FORTE:An ExistingSpace-based EHE Neutrino& Cosmic Ray Radio Detector?

  • Fast On-orbit Radio Transient Expt.

  • Pegasus launch in 1997

    • 800 km orbit, 3 year planned life

    • Testbed for non-proliferation & verification sensing

    • Dept. of Energy funded, LANL & Sandia construction & operation

    • Scientific program in lightning & related atmospheric discharges

  • 30-300MHz range, dual 20 MHz bands, 16 1MHz trigger channels

    • ~2M triggers recorded to date

  • FORTE can trigger on radio emission from Giant air showers E~100 EeV

  • Preliminary estimates: could be ~50-100 100 EeV cosmic ray events in sample

    • Analysis (UH, JPL, LANL) in progress; limits soon.


Limits from forte and glue
Limits from FORTE and GLUE

see astro/ph0309656 and astro/ph0310232


Antarctic impulsive transient antenna anita
Antarctic Impulsive Transient Antenna (ANITA)

  • ANITA Goal: Pathfinding mission for ultra-high energy cosmic neutrinos.

  • Science team: P. Gorham (PI), S. Barwick (UCI), J. Beatty, S. Coutu (Penn State), P. Evenson, J. Clem, D. Seckel (U.Del./Bartol), F. Halzen (Wisconsin), D. Kieda (Utah), J. Learned (UH), D. Saltzberg (UCLA), K. Liewer, S. Lowe, C. Naudet (JPL), A. Jacobson (LANL)

M. Rosen, Univ. of Hawaii

Solar

Panels

ANITA

Gondola &

Payload

Cover (partially cut away)

Antenna array


Anita radio from eev s in polar ice
ANITARadio from EeV ν’s in Polar Ice

• NASA approved 2002

•Successful test flight 1/04

• Data in 2007

Peter Gorham, UH


Radio Detection in Natural Salt DomesSALSA

  • Natural salt can be extremely low RF loss: ~ as clear as very cold ice, but nearly 2.5 times as dense.

  • Typical salt dome halite is comparable to ice at -40C for RF clarity.

5-10km

SALT curves are for (top): purest natural salt; (middle): typical good salt dome; (bottom) best salt bed halite. New measurements 2001, SLAC 2002.

P. Gorham

3-5 km


Ashra new project combining air cherenkov and fluorescence detection
ASHRANew Project Combining Air Cherenkov and Fluorescence Detection

$0.04/pixel

M. Sasaki U. Tokyo ICRR

Test Telescope on Haleakala in ‘03


RICE

AGASA

Amanda, Baikal

2002

Anita

2004

AUGER nt

AABN

2007

EUSO,

OWL,

ASHRA

2012

Auger

Salsa

km3

High Energy Neutrino Astronomy Coming Soon!

GLUE

projection by Christian Spiering, 10/02


ad